Kavli Affiliate: Dheeraj R. Pasham
| First 5 Authors: Daniel A. Paradiso, Eric R. Coughlin, Jonathan Zrake, Dheeraj R. Pasham,
| Summary:
Observations and theory suggest that core-collapse supernovae can span a
range of explosion energies, and when sub-energetic, the shockwave initiating
the explosion can decelerate to speeds comparable to the escape speed of the
progenitor. In these cases, gravity will complicate the explosion hydrodynamics
and conceivably cause the shock to stall at large radii within the progenitor
star. To understand these unique properties of weak explosions, we develop a
perturbative approach for modeling the propagation of an initially strong shock
into a time-steady, infalling medium in the gravitational field of a compact
object. This method writes the shock position and the post-shock velocity,
density, and pressure as series solutions in the (time-dependent) ratio of the
freefall speed to the shock speed, and predicts that the shock stalls within
the progenitor if the explosion energy is below a critical value. We show that
our model agrees very well with hydrodynamic simulations, and accurately
predicts (e.g.) the time-dependent shock position and velocity and the radius
at which the shock stalls. Our results have implications for black hole
formation and the newly detected class of fast X-ray transients (FXTs). In
particular, we propose that a “phantom shock breakout” — where the outer
edge of the star falls through a stalled shock — can yield a burst of X-rays
without a subsequent optical/UV signature, similar to FXTs. This model predicts
the rise time of the X-ray burst, $t_{rm d}$, and the mean photon energy,
$kT$, are anti-correlated, approximately as $T propto t_{rm d}^{-5/8}$.
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